J/A+A/708/A267 THU SESNe spectra (Xiang+, 2026)
Spectral dataset of stripped-envelope supernovae from the
Tsinghua supernova group.
Xiang D., Wang X., Zhang J., Yan S., Lin H., Rui L., Mo J., Zhang X.,
Sai H., Miao C., Xi G., Chen Z., Guo F., Ma X., Li G., Zhang T., Chen L.,
Liu J., Li W., Zhao X., Huang F., Cai Y., Lin W., Lin J., Wu C., Hu M.,
Song C., Zhang J., Xia Q., Li Z., Li L., Zhang K., Zhai Q., Chen J.,
Fan Z., Fu J., Qian S., Wu H., Wu X.-B., Yan J., Zhang H., Zhang J.,
Zhang L., Zheng J.
<Astron. Astrophys. 708, A267 (2026)>
=2026A&A...708A.267X 2026A&A...708A.267X (SIMBAD/NED BibCode)
ADC_Keywords: Supernovae ; Spectroscopy
Keywords: methods: data analysis - techniques: spectroscopic - stars: massive -
supernovae: general
Abstract:
The extent of envelope stripping in the progenitor stars is directly
reflected in the diversity of spectral features observed in
stripped-envelope supernovae (SESNe). Through extensive spectral
observation and analysis, we aim to clarify the statistical
differences between the subclasses of SESNe. The Tsinghua Supernova
group obtained 249 optical spectra of 62 SESNe during the years from
2010 to 2020, covering phases from -16 to over 190 days relative to
maximum light. Most spectra were obtained during the photospheric
phases after the supernova explosion. For each spectrum, the
pseudo-equivalent widths (pEWs) and blueshift velocities of principal
lines were measured. We further investigated the common spectral
features by analysing their velocity and strength correlations across
all subtypes. We identify the feature near 6200Å in SNe Ib as
Hα through comparison with SNe IIb and Ic, which
resolves inconsistent literature interpretations. Our finding reveals
prevalent residual hydrogen in SNe Ib, further supporting a continuous
stripping sequence from SNe IIb to Ib. We observe a trend in
increasing velocity among different subtypes of stripped-envelope SNe,
with SNe IIb exhibiting the lowest line velocities, followed by Ib,
Ic, and Ic-BL. Typically, the O∼I lines in SNe Ic/Ic-BL are stronger
than those seen in SNe IIb/Ib. In nebular phases, the [CaII] emission
dominates over [OI] in SNe IIb/Ib while [OI] is stronger in SNe Ic,
including the He-rich SN 2016coi. This spectral dichotomy implies that
progenitors of SNe Ic (BL) have more massive CO cores and hence higher
initial masses.
Description:
A full table of the journal of spectroscopic observations of the THU
SESNe sample (Table A.2). And the Spearman's rank correlation
coefficients of the line parameters shown in Figures 12 and 13.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea2.dat 83 249 Journal of spectroscopic observations of
our SESNe sample
spear.dat 56 240 Data behind Figs. 12,13
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Byte-by-byte Description of file: tablea2.dat
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Bytes Format Units Label Explanations
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1- 23 A23 --- SN SN name
25- 34 A10 "date" UT-date UT date of observation
36- 45 F10.2 d JD Julian Date of observation
50- 55 F6.1 d Phase Restframe phase in days relative to
maximum light
58- 65 A8 --- Tel Name of the telescope (1)
74- 83 A10 0.1nm waveRange Wavelength Range in angtroms
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Note (1): Telescopes as follows:
LJT = the 2.4-m telescope at Lijiang Observatory
XLT = the 2.16-m telescope at Beijing Xinglong Observatory (BAO)
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Byte-by-byte Description of file: spear.dat
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Bytes Format Units Label Explanations
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1- 4 A4 --- Type SN type (1)
8- 18 A11 --- Param1 Parameter 1 of the correlation
20- 30 A11 --- Param2 Parameter 2 of the correlation
35- 40 F6.3 --- rho Spearman's rank correlation coefficient
42- 50 E9.3 --- p p-value of the correlation
54- 56 I3 --- N Number of data points in the correlation
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Note (1): The He-rich broadlined SN 2016coi is noted as type IbBL.
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Acknowledgements:
Danfeng Xiang, xiangdanfeng2015(at)163.com
License: CC-BY-4.0 [see https://spdx.org/licenses/]
(End) Patricia Vannier [CDS] 11-Mar-2026